CWNU 64

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0.02 UTI
0.0
CN
0.91
Cdens
0.5
CC3
0.0
Clit
0.08
Cdup
C3 classification BB
Number of members (P>50%) 24
Radius (P>50% members) 4.3 [arcmin]
  • CN 0.0 Sparse
  • Cdens 0.91 Very dense
  • CC3 0.5 Intermediate quality
  • Clit 0.0 Rarely studied
  • Cdup 0.08 Very likely duplicate
📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview
CWNU 64 is a sparse, very dense object of intermediate C3 quality. Its parallax locates it at a relatively close distance, below the mid-plane, affected by moderate extinction. It is catalogued as a metal-poor, intermediate-age cluster (see Parameters). It is rarely studied in the literature.

⚠️ Warning: This is very likely a duplicate object, which shares a large percentage of members with at least one previously reported entry, and a large percentage with at least one entry reported in the same catalogue. See table with shared members information.

Relatively close Moderate extinction Metal-poor Intermediate age

Data
Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC – 305.896 31.084 0.544 -2.11 -5.155 26.569
He et al. 2022 305.862 31.127 0.51 -2.01 -5.16 0.2

💡 Note: The UCC values are estimated from its identified members.

Reference Year Dist [kpc] Av [mag] DAv [mag] Age [Myr] [Fe/H] [dex] Mass [Msun] Bfr BSS
He et al. 2022 1.55 2.04 – 631 -0.642 – – –

💡 Note: The parameters are sometimes transformed from their original values to match the format of the columns shown here, see FAQ. The columns DAv, Bfr, BSS correspond to differential extinction, binary fraction, and blue stragglers, respectively. BSS values can be listed as fractions or integers.

Cluster % RA DEC Plx pmRA pmDE Rv UTI
CWNU 30 92.0 305.9 31.06 0.55 -2.13 -5.15 4.01 0.04
Theia 4509 92.0 305.9 31.06 0.55 -2.14 -5.15 4.01 0.02
UBC 1088 92.0 305.9 31.06 0.55 -2.13 -5.15 4.01 0.44

💡 Note: The % column shows the percentage of members that CWNU 64 shares with each listed object.

Visualization
CWNU 64 UCC
Galactocentric position diagram

💡 Note: How are the galactocentric plots generated? See FAQ.